dc.contributor.author | Meyer, DM-A | |
dc.contributor.author | Kreplin, A | |
dc.contributor.author | Kraus, S | |
dc.contributor.author | Vorobyov, EI | |
dc.contributor.author | Haemmerle, L | |
dc.contributor.author | Eisloeffel, J | |
dc.date.accessioned | 2019-06-10T07:58:46Z | |
dc.date.issued | 2019-06-10 | |
dc.description.abstract | Massive young stellar object (MYSOs) form during the collapse of high-mass pre-stellar cores, where infalling molecular material is accreted through a centrifugally-balanced accretion disc that is subject to efficient gravitational instabilities. In the resulting fragmented accretion disc of the MYSO, gaseous clumps and low-mass stellar companions can form, which will influence the future evolution of massive protostars in the Hertzsprung-Russell diagram. We perform dust continuum radiative transfer calculations and compute synthetic images of disc structures modelled by the gravito-radiation-hydrodynamics simulation of a forming MYSO, in order to investigate the Atacama Large Millimeter/submillimeter Array (ALMA) observability of circumstellar gaseous clumps and forming multiple systems. Both spiral arms and gaseous clumps located at ~a few 100 au from the protostar can be resolved by interferometric ALMA Cycle 7 C43-8 and C43-10 observations at band 6 (1.2 mm), using a maximal 0.015" beam angular resolution and at least 10-30 min exposure time for sources at distances of 1-2 kpc. Our study shows that substructures are observable regardless of their viewing geometry or can be inferred in the case of an edge-viewed disc. The observation probability of the clumps increases with the gradually increasing efficiency of gravitational instability at work as the disc evolves. As a consequence, large discs around MYSOs close to the zero-age-main-sequence line exhibit more substructures than at the end of the gravitational collapse. Our results motivate further observational campaigns devoted to the close surroundings of the massive protostars S255IR-NIRS3 and NGC 6334I-MM1, whose recent outbursts are a probable signature of disc fragmentation and accretion variability. | en_GB |
dc.description.sponsorship | European Research Council (ERC) | en_GB |
dc.description.sponsorship | Science and Technology Facilities Council (STFC) | en_GB |
dc.description.sponsorship | Russian Science Foundation | en_GB |
dc.description.sponsorship | Swiss National Science Foundation | en_GB |
dc.identifier.citation | Vol. 487 (4), pp. 4473-4491 | en_GB |
dc.identifier.doi | 10.1093/mnras/stz1585 | |
dc.identifier.grantnumber | 639889 | en_GB |
dc.identifier.grantnumber | ST/J004030/1 | en_GB |
dc.identifier.grantnumber | ST/K003445/1 | en_GB |
dc.identifier.grantnumber | 18-12-00193 | en_GB |
dc.identifier.grantnumber | 200020-172505 | en_GB |
dc.identifier.uri | http://hdl.handle.net/10871/37424 | |
dc.language.iso | en | en_GB |
dc.publisher | Oxford University Press (OUP) / Royal Astronomical Society | en_GB |
dc.rights | © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. | en_GB |
dc.subject | methods: numerical | en_GB |
dc.subject | radiative transfer | en_GB |
dc.subject | stars: circumstellar matter | en_GB |
dc.title | On the ALMA observability of nascent massive multiple systems formed by gravitational instability | en_GB |
dc.type | Article | en_GB |
dc.date.available | 2019-06-10T07:58:46Z | |
dc.identifier.issn | 0035-8711 | |
dc.description | This is the final version. Available from Oxford University Press via the DOI in this record. | en_GB |
dc.identifier.eissn | 1365-2966 | |
dc.identifier.journal | Monthly Notices of the Royal Astronomical Society | en_GB |
dc.rights.uri | http://www.rioxx.net/licenses/all-rights-reserved | en_GB |
dcterms.dateAccepted | 2019-06-05 | |
rioxxterms.version | VoR | en_GB |
rioxxterms.type | Journal Article/Review | en_GB |
refterms.dateFCD | 2019-06-07T12:15:23Z | |
refterms.versionFCD | AM | |
refterms.dateFOA | 2019-07-09T14:32:31Z | |
refterms.panel | B | en_GB |